Dark photon vortex formation and dynamics

East, William E.; Huang, Junwu

doi:10.1007/jhep12(2022)089

Cited by 18 publications

(2 citation statements)

References 77 publications

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“…An ultra-light dark photon is an essential ingredient in dark matter models, either as a light bosonic dark matter candidate [21][22][23], or as a mediator to a sector of dark matter particles (see [24] and reference within). Despite recent evidence of various collective effects which cast doubt on the validity of some of the models (vortex production during production of dark photon dark matter [25] and the two stream instability in the case of freeze-in dark matter models [26]), it is still of great interest to probe the existence of ultra-light dark photons regardless of their cosmological abundance through superradiance [25,[27][28][29][30], cosmology [31][32][33][34], stellar objects [35][36][37] and lab searches [38][39][40][41][42].…”

Section: Jcap01(2024)019 1 Introductionmentioning

confidence: 99%

Patchy screening of the CMB from dark photons

Pîrvu,

Huang,

Johnson

2024

J. Cosmol. Astropart. Phys.

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We study anisotropic (patchy) screening induced by the resonant conversion of cosmic microwave background (CMB) photons into dark-sector massive vector bosons (dark photons) as they cross non-linear large scale structure (LSS). Resonant conversion takes place through the kinetic mixing of the photon with the dark photon, one of the simplest low energy extensions to the Standard Model. In the early Universe, resonant conversion can occur when the photon plasma mass, obtained as the photon propagates through the ionized interstellar and intergalactic media, matches the dark photon mass. After the epoch of reionization, resonant conversion occurs mainly in the ionized gas that occupies virialized dark matter halos, for a range of dark photon masses between 10-13 eV ≲ m A' ≲ 10-11 eV. This leads to new CMB anisotropies that are correlated with LSS, which we refer to as patchy dark screening, in analogy with anisotropies from Thomson screening. Its unique frequency dependence allows it to be distinguished from the blackbody CMB. In this paper, we use a halo model approach to predict the imprint of dark screening on the CMB temperature and polarization anisotropies, as well as their correlation with LSS. We then examine the two- and three-point correlation functions of the dark-screened CMB, as well as correlation functions between CMB and LSS observables, to project the sensitivity of future measurements to the kinetic mixing parameter and dark photon mass. We demonstrate that an analysis with existing CMB data can improve upon current constraints on the kinetic mixing parameter by two orders of magnitude with the two-point correlation functions, while data from upcoming CMB experiments and LSS surveys can further improve the reach by another order of magnitude with two- and three-point correlation functions.

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Section: Jcap01(2024)019 1 Introductionmentioning

confidence: 99%

Patchy screening of the CMB from dark photons

Pîrvu,

Huang,

Johnson

2024

J. Cosmol. Astropart. Phys.

Self Cite

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“…Dark photons being the gauge boson of an extra U (1) group that couples to the Standard Model sector are well motivated in string theory compactifications [482,483,484,49,485], which may kinetically mix with Standard Model photons [51,486,487]. Sufficiently long-lived dark photon with a mass m A can be produced through a number of mechanisms, including inflationary fluctuations [481,488,489,490], tachyonic instability [491,492,493] and parametric resonance [494], the misalignment mechanism [480,495], or cosmic strings [496,497], and constitute part of or all the cosmological dark matter. A wide variety of experiments constrain the dark photon dark matter parameter space, including Figure 40: Constraints on the interaction parameter in Eq.…”

Section: Introductionmentioning

confidence: 99%

Feebly-interacting particles: FIPs 2020 workshop report

et al. 2021

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With the establishment and maturation of the experimental programs searching for new physics with sizeable couplings at the LHC, there is an increasing interest in the broader particle and astrophysics community for exploring the physics of light and feebly-interacting particles as a paradigm complementary to a New Physics sector at the TeV scale and beyond. FIPs 2020 has been the first workshop fully dedicated to the physics of feebly-interacting particles and was held virtually from 31 August to 4 September 2020. The workshop has gathered together experts from collider, beam dump, fixed target experiments, as well as from astrophysics, axions/ALPs searches, current/future neutrino experiments, and dark matter direct detection communities to discuss progress in experimental searches and underlying theory models for FIPs physics, and to enhance the cross-fertilisation across different fields. FIPs 2020 has been complemented by the topical workshop “Physics Beyond Colliders meets theory”, held at CERN from 7 June to 9 June 2020. This document presents the summary of the talks presented at the workshops and the outcome of the subsequent discussions held immediately after. It aims to provide a clear picture of this blooming field and proposes a few recommendations for the next round of experimental results.

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Early vs late string networks from a minimal QCD Axion

Gorghetto,

Hardy,

Nicolaescu

et al. 2024

J. High Energ. Phys.

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We propose a new regime of minimal QCD axion dark matter that lies between the pre- and post-inflationary scenarios, such that the Peccei-Quinn (PQ) symmetry is restored only on sufficiently large spatial scales. This leads to a novel cosmological evolution, in which strings and domain walls re-enter the horizon and annihilate later than in the ordinary post-inflationary regime, possibly even after the QCD crossover. Such dynamics can occur if the PQ symmetry is restored by inflationary fluctuations, i.e. the Hubble parameter during inflation HI is larger than the PQ breaking scale fa, but it is not thermally restored afterwards. Solving the Fokker-Planck equation, we estimate the number of inflationary e-folds required for the PQ symmetry to be, on average, restored. Moreover, we show that, in the large parts of parameter space where the radial mode is displaced from the minimum by de Sitter fluctuations, a string network forms due to the radial mode oscillating over the top of its potential after inflation. In both cases we identify order one ranges in HI/fa and in the quartic coupling λ of the PQ potential that lead to the late-string dynamics. In this regime the cosmological dark matter abundance can be reproduced for axion decay constants as low as the astrophysical constraint 𝒪(108) GeV, corresponding to axion masses up to 10−2 eV, and with miniclusters with masses as large as 𝒪(10)M⊙.

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Dark photon vortex formation and dynamics

Cited by 18 publications

References 77 publications

Patchy screening of the CMB from dark photons

Patchy screening of the CMB from dark photons

Feebly-interacting particles: FIPs 2020 workshop report

Early vs late string networks from a minimal QCD Axion

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